SN2012ab: a peculiar Type IIn supernova with aspherical circumstellar material
Williams, G Grant
Graham, Melissa L
Mauerhan, Jon C
Andrews, Jennifer E
Filippenko, Alexei V
Hoffman, Jennifer L
Leonard, Douglas C
Marion, G H
Milne, P. A.
Quimby, Robert M
Silverman, Jeffrey M
Wheeler, J Craig
AffiliationUniv Arizona, Steward Observ
Keywordssupernovae: individual: Type IIn
MetadataShow full item record
PublisherOXFORD UNIV PRESS
CitationChristopher Bilinski, Nathan Smith, G Grant Williams, Paul Smith, WeiKang Zheng, Melissa L Graham, Jon C Mauerhan, Jennifer E Andrews, Alexei V Filippenko, Carl Akerlof, E Chatzopoulos, Jennifer L Hoffman, Leah Huk, Douglas C Leonard, G H Marion, Peter Milne, Robert M Quimby, Jeffrey M Silverman, Jozsef Vinkó, J Craig Wheeler, Fang Yuan; SN2012ab: a peculiar Type IIn supernova with aspherical circumstellar material, Monthly Notices of the Royal Astronomical Society, Volume 475, Issue 1, 21 March 2018, Pages 1104–1120, https://doi.org/10.1093/mnras/stx3214
Rights© 2017 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society
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AbstractWe present photometry, spectra, and spectropolarimetry of supernova (SN) 2012ab, mostly obtained over the course of similar to 300 d after discovery. SN 2012ab was a Type IIn (SN IIn) event discovered near the nucleus of spiral galaxy 2MASXJ12224762+0536247. While its light curve resembles that of SN 1998S, its spectral evolution does not. We see indications of CSM interaction in the strong intermediate-width emission features, the high luminosity (peak at absolute magnitude M = -19.5), and the lack of broad absorption features in the spectrum. The Ha emission undergoes a peculiar transition. At early times it shows a broad blue emission wing out to -14000 km s(-1) and a truncated red wing. Then at late times (> 100 d) it shows a truncated blue wing and a very broad red emission wing out to roughly +20 000 km s(-1). This late-time broad red wing probably arises in the reverse shock. Spectra also show an asymmetric intermediate-width H alpha component with stronger emission on the red side at late times. The evolution of the asymmetric profiles requires a density structure in the distant CSM that is highly aspherical. Our spectropolarimetric data also suggest asphericity with a strong continuum polarization of similar to 1-3 per cent and depolarization in the Ha line, indicating asphericity in the CSM at a level comparable to that in other SNe IIn. We estimate a mass-loss rate of M = 0.050 M-circle dot yr(-1) for v(pre) = 100 km s(-1) extending back at least 75 yr prior to the SN. The strong departure from axisymmetry in the CSM of SN 2012ab may suggest that the progenitor was an eccentric binary system undergoing eruptive mass loss.
VersionFinal published version
SponsorsNSF [AST-1210599, AST-1312221, AST-1515559, AST-1211916, AST-1109881, PhY-0801007, AST-1009571, AST-1210311]; Research Corporation for Science Advancement; NSF Astronomy and Astrophysics Postdoctoral Fellowship [AST-1302771]; TABASGO Foundation; Gary and Cynthia Bengier; Christopher R. Redlich Fund; Richard & Rhoda Goldman Fund; Miller Institute for Basic Research in Science (U.C. Berkeley); NASA [NNX08AV63G]; Australian Research Council; University of New South Wales; University of Texas; University of Michigan; W.M. Keck Foundation